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A Method for Estimating the Number of Regolith Particles in a Dust Cloud in a Discharge Initiated by Gyrotron Radiation 估计由陀螺辐射引发的放电中尘埃云中碎石颗粒数量的方法
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700379
A. S. Sokolov, T. E. Gayanova, A. K. Kozak, D. V. Malakhov, I. R. Nugaev, D. E. Kharlachev, V. D. Stepakhin
{"title":"A Method for Estimating the Number of Regolith Particles in a Dust Cloud in a Discharge Initiated by Gyrotron Radiation","authors":"A. S. Sokolov,&nbsp;T. E. Gayanova,&nbsp;A. K. Kozak,&nbsp;D. V. Malakhov,&nbsp;I. R. Nugaev,&nbsp;D. E. Kharlachev,&nbsp;V. D. Stepakhin","doi":"10.1134/S1063772924700379","DOIUrl":"10.1134/S1063772924700379","url":null,"abstract":"<p>The article proposes a new method for estimating the number of particles in experiments on modeling the interaction of cosmic and lunar dust with the surface of spacecraft. The experiments are based on the creation of a dusty plasma cloud, when exposed to radiation from a powerful pulsed gyrotron on a substance simulating cosmic or lunar dust. This approach was tested using a lunar regolith simulator. The dynamics of particles in dust clouds obtained as a result of microwave discharge is analyzed using the ImageJ program.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"388 - 394"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141785620","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Study of the Magnetic Reconnection Effect in a Laboratory Astrophysical Experiment on X-Ray L-Shell Emission Spectra of Multicharged Ions 实验室天体物理实验中对多充离子 X 射线 L 壳发射光谱的磁重联效应研究
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700331
M. A. Alkhimova, S. S. Makarov, I. Yu. Skobelev, S. N. Ryazantsev, E. D. Filippov
{"title":"Study of the Magnetic Reconnection Effect in a Laboratory Astrophysical Experiment on X-Ray L-Shell Emission Spectra of Multicharged Ions","authors":"M. A. Alkhimova,&nbsp;S. S. Makarov,&nbsp;I. Yu. Skobelev,&nbsp;S. N. Ryazantsev,&nbsp;E. D. Filippov","doi":"10.1134/S1063772924700331","DOIUrl":"10.1134/S1063772924700331","url":null,"abstract":"<p>In the paper, we demonstrate the application of X-ray spectroscopy with high spatial resolution to study magnetic reconnection in laboratory astrophysical experiments performed with nano- and pico-second duration laser facilities at a moderate laser density on the target of &lt;10<sup>18</sup> W/cm<sup>2</sup>. A brief overview of the commonly used experimental schemes is given. Atomic kinetic calculations for the L-shell spectra of Ne- and F‑like Fe ions (iron, <i>Z</i> = 26) demonstrate the high sensitivity of the measurements to changes in plasma parameters. The scope of the different diagnostic approaches to measure electron temperature and laser plasma density is discussed. It is shown that transitions in Ne-like ions are a universal tool for measuring plasma parameters, both in the region of laser interaction with the target and in the reconnection zone.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"345 - 355"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141776977","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Simulation of Astrophysical Jets in Magnetic Fields of Laser Relativistic Plasmas 激光相对论等离子体磁场中的天体物理喷流模拟
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700343
V. S. Belyaev, V. P. Krainov, A. P. Matafonov
{"title":"Simulation of Astrophysical Jets in Magnetic Fields of Laser Relativistic Plasmas","authors":"V. S. Belyaev,&nbsp;V. P. Krainov,&nbsp;A. P. Matafonov","doi":"10.1134/S1063772924700343","DOIUrl":"10.1134/S1063772924700343","url":null,"abstract":"<p>A brief review of the results of experimental modeling of cosmic jets in superstrong magnetic fields of laser relativistic plasma is given. It is noted that the development of cyclotron instability with the generation of cyclotron radiation plays a key role in a number of processes in a plasma with a magnetic field: self-localization of plasma in the form of solitons, conversion of rotational motion of plasma into translational motion, cyclotron acceleration of charged particles, and separation (stratification) of a plasma jet into separate plasma formations.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"356 - 364"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141785619","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
MHD Simulations of Astrophysical and Laboratory Jets under Different Magnetic Field Configurations 不同磁场配置下天体物理和实验室喷流的 MHD 模拟
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700380
O. D. Toropina, G. S. Bisnovatyi-Kogan, S. G. Moiseenko
{"title":"MHD Simulations of Astrophysical and Laboratory Jets under Different Magnetic Field Configurations","authors":"O. D. Toropina,&nbsp;G. S. Bisnovatyi-Kogan,&nbsp;S. G. Moiseenko","doi":"10.1134/S1063772924700380","DOIUrl":"10.1134/S1063772924700380","url":null,"abstract":"<p>This paper presents the results of MHD simulations of astrophysical and laboratory supersonic jets under a superposition of poloidal (<span>({{B}_{r}})</span>, <span>({{B}_{z}})</span>) and toroidal (<span>({{B}_{phi }})</span>) magnetic fields. It is shown that the escaping matter is quickly collimated by the magnetic field. A shock wave of an elongated shape is formed, which moves from the target to the boundary of the chamber, leaving behind a stable flow. A periodic shock wave structure is observed inside the main conical expanding shock wave. It is shown that the toroidal component of the magnetic field remains in the region throughout the entire calculation and plays a role in the collimation of the flow. The poloidal magnetic field decreases in the region of the jet cone, but remains in the simulation region throughout the calculation and also participates in flow collimation. Thus, both components <span>({{B}_{z}})</span> and <span>({{B}_{phi }})</span> take part in the collimation of the flow by the magnetic field. The width of the jet and the opening angle of the cone <span>(theta )</span> depend on the magnitude of the magnetic field induction. As the field increases, the jet becomes narrower and the cone angle decreases. Initially, we do not specify the rotation of the jet <span>(Omega )</span>. However, due to the presence of the <span>({{B}_{phi }})</span> field, the substance acquires angular velocity and twists along the <span>(z)</span> axis. The simulation results are in agreement with laboratory jets arising in the experiment at the Neodymium laser installation, and with the previously obtained results of MHD modeling of jet formation separately, in poloidal or toroidal magnetic field.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"395 - 405"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141776982","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Hall Effects and Diamagnetic Cavity Collapse during a Laser Plasma Cloud Expansion into a Vacuum Magnetic Field 激光等离子体云扩展到真空磁场过程中的霍尔效应和二磁腔塌陷
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700409
A. A. Chibranov, I. F. Shaikhislamov, A. G. Berezutskiy, V. G. Posukh, P. A. Trushin, Yu. P. Zakharov, I. B. Miroshnichenko, M. S. Rumenskikh, V. A. Terekhin
{"title":"Hall Effects and Diamagnetic Cavity Collapse during a Laser Plasma Cloud Expansion into a Vacuum Magnetic Field","authors":"A. A. Chibranov,&nbsp;I. F. Shaikhislamov,&nbsp;A. G. Berezutskiy,&nbsp;V. G. Posukh,&nbsp;P. A. Trushin,&nbsp;Yu. P. Zakharov,&nbsp;I. B. Miroshnichenko,&nbsp;M. S. Rumenskikh,&nbsp;V. A. Terekhin","doi":"10.1134/S1063772924700409","DOIUrl":"10.1134/S1063772924700409","url":null,"abstract":"<p>This paper describes the results of a laboratory experiment on the sub-Alfvén expansion of a quasi-spherical laser plasma cloud into a vacuum magnetic field in the regime of nonmagnetized ions. The role of Hall fields and currents in the anomalously fast dynamics of the magnetic field during the collapse phase of a diamagnetic cavity is considered. Detailed spatial measurements of the azimuthal Hall fields configuration are demonstrated and their relationship to diamagnetic cavity collapse is determined. As a result of the experiment, data were obtained confirming the hypothesis about the transfer of the main magnetic field by the movement of electrons associated with Hall currents.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"418 - 428"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141776983","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Dynamics of the Plasma Ejection Structure in Laboratory Modeling of Young Star Jets at Plasma Focus Facilities 等离子体聚焦设施年轻恒星喷流实验室建模中的等离子体喷射结构动力学
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-27 DOI: 10.1134/S1063772924700355
I. Yu. Kalashnikov, V. S. Beskin, V. I. Krauz
{"title":"Dynamics of the Plasma Ejection Structure in Laboratory Modeling of Young Star Jets at Plasma Focus Facilities","authors":"I. Yu. Kalashnikov,&nbsp;V. S. Beskin,&nbsp;V. I. Krauz","doi":"10.1134/S1063772924700355","DOIUrl":"10.1134/S1063772924700355","url":null,"abstract":"<p>The use of “plasma focus” type facilities, such as PF-3 (Kurchatov Institute), allows carrying out well-controlled and diagnosable laboratory experiments to study laboratory jets with scale parameters close to the jets of young stars. In this paper, we present the results of numerical modeling of plasma outburst propagation in PF-3. A self-consistent configuration was chosen as the initial conditions, which correctly describes the internal structure of the jet. This allowed us to obtain a detailed structure of the interaction between the magnetized emission and the ambient gas. Due to the scalability of such a structure, one should expect such a structure from the head shock waves of jets of young stars.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 4","pages":"365 - 376"},"PeriodicalIF":1.1,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141776980","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Probing the Ionosphere with Pulses from the Pulsar B2016+28 at a Frequency of 324 MHz 利用脉冲星 B2016+28 发出的频率为 324 兆赫的脉冲探测电离层
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-04 DOI: 10.1134/S1063772924700276
M. S. Burgin, M. V. Popov
{"title":"Probing the Ionosphere with Pulses from the Pulsar B2016+28 at a Frequency of 324 MHz","authors":"M. S. Burgin,&nbsp;M. V. Popov","doi":"10.1134/S1063772924700276","DOIUrl":"10.1134/S1063772924700276","url":null,"abstract":"<p>Using ground-space VLBI data from the RadioAstron project archive, the phase distortions of the cross-spectrum caused by the ionosphere have been calculated and their influence on the results of determination of the visibility function has been studied. The Arecibo Observatory’s 300-m antenna served as the ground station for the interferometer. The separation of ionospheric phase distortions from the influence of the interstellar and interplanetary medium and instrumental errors is based on different frequency dependencies of these effects. The amplitude of ionospheric phase variation caused by electron density fluctuations in the ionosphere above the Arecibo radio telescope is several radians per observation session of about one hour. The structure function of phase variations indicates a continuous spectrum of electron density fluctuations at typical times of <span>( gtrsim )</span>2–5 min with no pronounced signs of quasi-periodic processes. Ionospheric phase f-luctuations during pulsar observations increase the width of the maximum of the amplitude of the visibility function as a function of the residual fringe rate by 5–10 mHz with a decrease in the value at the maximum of <span>( approx {kern 1pt} 10% )</span>. When constructing images of radio galaxies and quasars from ground-based VLBI observations, these phase shifts can significantly distort the final results.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 3","pages":"257 - 267"},"PeriodicalIF":1.1,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141547218","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Estimation of the Spin of a Supermassive Black Hole in Sagittarius A* 人马座 A* 中超大质量黑洞的自旋估计
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-04 DOI: 10.1134/S106377292470032X
A. S. Andrianov, S. V. Chernov
{"title":"Estimation of the Spin of a Supermassive Black Hole in Sagittarius A*","authors":"A. S. Andrianov,&nbsp;S. V. Chernov","doi":"10.1134/S106377292470032X","DOIUrl":"10.1134/S106377292470032X","url":null,"abstract":"<p>In April 2017, the Event Horizon telescope received an image of a supermassive black hole in the Sagittarius <i>A</i>* source. This image consists of a ring-like structure that contains three areas with increased brightness (spots). If we assume that these spots are associated with flares near the event horizon of a black hole, then we can estimate its spin. Our estimate gives a value of the order of <span>(a approx 0.9)</span>.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 3","pages":"233 - 237"},"PeriodicalIF":1.1,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S106377292470032X.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141547219","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
National Software for Processing Information of the Satellite–Satellite Space Geodetic System 处理卫星-卫星空间大地测量系统信息的国家软件
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-04 DOI: 10.1134/S1063772924700288
A. S. Zhamkov, S. V. Ayukov, A. I. Filetkin, V. K. Milyukov, I. Yu. Vlasov, V. N. Sementsov, I. V. Gusev, V. E. Zharov
{"title":"National Software for Processing Information of the Satellite–Satellite Space Geodetic System","authors":"A. S. Zhamkov,&nbsp;S. V. Ayukov,&nbsp;A. I. Filetkin,&nbsp;V. K. Milyukov,&nbsp;I. Yu. Vlasov,&nbsp;V. N. Sementsov,&nbsp;I. V. Gusev,&nbsp;V. E. Zharov","doi":"10.1134/S1063772924700288","DOIUrl":"10.1134/S1063772924700288","url":null,"abstract":"<p>The paper presents the principle of operation, the main components and the results of the work of the software created in the Sternberg Astronomical Institute of Moscow State University. The PC is designed for processing of large volumes of space geodetic data. The developed software was used to process inter-satellite measurements of a space-based constellation intended to measure the parameters of the Earth’s gravitational field (EGF). The experimental option of the software enables working with both simulated data and real data of GRACE and GRACE Follow-on missions. This experimental version was used to recover the EGF parameters on real GRACE and GRACE-FO mission data. Solutions were developed for every month within the measurement time intervals from 2010 to 2021, as well as for extended time intervals of 4.3 and 7.6 years. A comparison of the obtained solutions with the results of the EGF recovery obtained by other researchers is presented.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 3","pages":"320 - 330"},"PeriodicalIF":1.1,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141547170","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Estimation of Pulsar’s Initial Spin by the Magnetic Dipole Radiation and Wind Model 利用磁偶极子辐射和风模型估算脉冲星的初始自旋
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-07-04 DOI: 10.1134/S1063772924700239
Yihong Sun, Dehua Wang, Chengmin Zhang, Jing Yu, Yungang Zhou, Ziyi You, Xianghan Cui, Jianwei Zhang
{"title":"Estimation of Pulsar’s Initial Spin by the Magnetic Dipole Radiation and Wind Model","authors":"Yihong Sun,&nbsp;Dehua Wang,&nbsp;Chengmin Zhang,&nbsp;Jing Yu,&nbsp;Yungang Zhou,&nbsp;Ziyi You,&nbsp;Xianghan Cui,&nbsp;Jianwei Zhang","doi":"10.1134/S1063772924700239","DOIUrl":"10.1134/S1063772924700239","url":null,"abstract":"<p>The estimation of the initial spin period of pulsars involves the important questions such as the late stage evolution of massive stars and the formation process of neutron stars. However, the estimated initial spin exists the bias based on the magnetic dipole radiation (MDR) model, since the braking index of a dozen of observed pulsars ranges in <span>(1 &lt; n &lt; 3)</span> that is deviated from the expected value of 3 by MDR. The magnetic dipole radiation plus wind (MDRW) model for a pulsar successfully explains the evolution of the braking index between 1 and 3, by which we calculate the initial spins of the pulsars with the measured braking index, and obtain their distribution between <span>( sim {kern 1pt} 18)</span> and <span>( sim {kern 1pt} 50)</span> ms. This result is consistent with the statistics of the observed young pulsars, less than the fastest spin period of 16 ms of the rotation-powered X-ray pulsar PSR J0537–6910.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 3","pages":"268 - 276"},"PeriodicalIF":1.1,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141547214","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
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